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I have edited some earlier versions of this article and had been monitoring it for bad edits, but I am leaving the WP and am now abandoning this article to its fate.

Just wanted to provide notice that I am only responsible (in part) for the last version I edited; see User:Hillman/Archive. I emphatically do not vouch for anything you might see in more recent versions, although I hope for the best.

Good luck in your search for information, regardless!---CH 02:38, 1 July 2006 (UTC)

Would someone knowledgeable comment on the spherically symmetric case, which parameters can be ignored, or other simplifications? And, for example, it appears that for GR that 4Φ1 + 4Φ2 + 2Φ3 + 6Φ4 + O(ε³) must add exactly to 2U² but this is very non-obvious. And if one had an alternate g00 for a symmetric metric, say either of the two common approximations g00 = -1/(1+U)^2 or g00 = -(1-U)^2, which parameters would these affect and by how much? I.e. how much suffers by our common approximations? Have we verified gravity that closely yet? Also, I personally feel this article should be raised in priority. Verification of gravity is a popular topic in the scientific press. But no one can get beyond superficial press talk, in part because the criteria, i.e. the PPN, are not given accessible explanations. Even Misner-Thorne-Wheeler text just says that calculating these is difficult and doesn't give, for example, ways to approximate the parameters. At one time 1st order was fine, but now we need accessibility to at least 2nd order in the PPN that is widely understood. Thanks. Rlshuler (talk) 21:57, 6 October 2015 (UTC)

Why the changes? First of all, μ{\displaystyle \mu } and ν{\displaystyle \nu } are the indexes, not i{\displaystyle i} and j{\displaystyle j}. This is because μ{\displaystyle \mu } and ν{\displaystyle \nu } follow the "g{\displaystyle g}" for the metric tensor. That makes μ{\displaystyle \mu } and ν{\displaystyle \nu } the indexes by definition. See tensor index notation about this.

Secondly, metric tensors in GR apply to spacetime (a combination of both space and time) and not just space. This because space and time are interchangeable in relativity. See special relativity and relativity of simultaneity for details. In fact, the result of integrating the metric tensor over a world lineW{\displaystyle W} via

Finally, a 4x4 metric requires that the indexes have 4 possible values. "1 to 3" is only 3 possible values. The modern convention is to number the coordinate time index as 0. Hence my statement that the indexes go from 0 to 3. EMS | Talk 00:16, 30 December 2017 (UTC)

The text in the next section refers to g00{\displaystyle g_{00}}, g0i{\displaystyle g_{0i}}, and gij{\displaystyle g_{ij}}. These mean the time-time component, the mixed time-space components, and the purely spatial components. See Ricci calculus#Space and time coordinates.

This article is not about Einstein's general relativity in its full generality with arbitrary curvilinear coordinates. It is about a quasi-classical approximation to any of large group of theories of which GTR is only one. It assumes that the coordinate system is nearly that of an inertial frame of reference, that is, a Cartesian coordinate system which is non-rotating and free-falling. JRSpriggs (talk) 06:12, 30 December 2017 (UTC)

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